Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...333..236k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 333, Oct. 1, 1988, p. 236-247.
Astronomy and Astrophysics
Astrophysics
195
Angular Momentum, Stellar Mass Ejection, Stellar Models, Stellar Rotation, Stellar Winds, Pre-Main Sequence Stars, Stellar Evolution, Stellar Interiors, Stellar Magnetic Fields
Scientific paper
The wind models discussed by Mestel (1984) are used here to formulate a general expression for the rate of angular momentum loss by magnetic stellar winds as a function of magnetic field configuration, rotation rate, and stellar model properties. The sensitivity of the rotation velocity to the various wind model parameters, the initial angular momenta, and the time dependence of the angular velocity for each mass is shown. The theoretical results are compared with observational ones, and it is found that the existence of very rapidly rotating stars in young clusters implies that low-mass stars are formed with a large spread of angular momentum. The high efficiency of angular momentum loss through magnetic stellar winds causes the rotation velocity to become less dependent on initial angular momentum J0 with time; by 300 million yur, the rotation velocity becomes independent of J0. This results in a decrease with time in the spread of rotation velocities as a function of stellar mass in young clusters.
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